LAMBDA News
Wilkinson Microwave Anisotropy Probe
Description
The TE, BB, and EE power spectra are computed using a pseudo-Cl estimator for the region outside the 5yr polarization mask in P and outside the analysis mask in T. The foreground-cleaned V band with uniform weighting is used for T. The combined foreground-cleaned Q and V bands are used for P. Polarization weighting uses the full Ninv weighting for l ≤ 16 and Nobs weighting for l > 16.
Unbinned TE, BB, and EE power spectra are provided as a tables containing the following three columns:
- the multipole moment l
- the power spectrum in units of μK2
- the corresponding diagonal elements of the covariance matrix
The diagonal elements provide an estimate of the error, but should not be used as exact error bars. The complete Fisher matrix should be used for that purpose.
Binned versions of the TE, BB, and EE power spectra is also available in separate ASCII file with the following columns:
- the mean multipole moment l
- the smallest l contributing to the bin
- the largest l contributing to the bin
- the power spectrum in units of μK2
- the corresponding diagonal elements of the covariance matrix
The BB and EE spectra bins are noise-weighted averages; the TE spectra bins are straight averages.
Binned versions of spectra for TE, BB, EE, TB, and EB containing only low l (l < 24) data are coming soon!
Additional Information
- Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Data Processing, Sky Maps, and Basic Results, G. Hinshaw, et.al. (2008)
- Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Likelihoods and Parameters from WMAP Data, J. Dunkley, et.al (2008).
- Five-Year Wilkinson Microwave Anisotropy Probe (WMAP) Observations: Angular Power Spectra, M. Nolta, et.al (2008).
- WMAP Five Year Explanatory Supplement
